Analysis of Balmer Lines Intensities and Radiation Non-Isotropy of SS 433 Jets

Panferov, A. A.; Fabrika, S.; Бычкова, Л. В.

doi:10.1007/978-94-011-1924-5_34

Cited by 9 publications

(11 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Middleton et al (2018) estimates that the intrinsic X-ray luminosity is L X 10 38 erg s −1 . This is consistent with our upper limits as long as the X-ray radiation is slightly less collimated ( 5 • ) than the beam containing the optical bullets, which is almost certainly the case from the presence of older jet knots that keep radiating for a few days (Panferov & Fabrika 1993).…”

Section: Collimated Radiationsupporting

confidence: 90%

“…We note that several related calculations to estimate the properties of the optical jets can be found in previous papers (e.g., Davidson & McCray 1980;Begelman et al 1980;Bodo et al 1985;Brown et al 1991;Panferov & Fabrika 1993), primarily based on the Hα luminosity. These calculations have several uncertainties: unknown heating mechanism and emission line emissivity, degeneracy between density and volume filling factor, unknown extinction, optical depth effects, unknown spatial emission profile of the optical jets (e.g., jet size).…”

Section: Resultsmentioning

confidence: 82%

“…where I(r 0 ) is the intensity at the base of the beam. The total luminosity in the collimated radiation could be higher if it is broader than the beam containing the optical bullets, which is likely the case from the presence of older jet knots that can keep radiating for a few days (Panferov & Fabrika 1993). 5.…”

Section: Cloudy Models For Photoionized Optical Bulletsmentioning

confidence: 99%

“…The optical bullets that make up the optical jets are thought to form from the collapse of gas from the continuous X-ray jet through a thermal instability as the jet expands and cools (Davidson & McCray 1980;Brinkmann et al 1988). If the optical bullets are heated mainly by photoionization by collimated radiation (Bodo et al 1985;Panferov & Fabrika 1993), they can serve as a probe of the latter. On the other hand, their heating has generally been ascribed to external processes related to interaction with the ambient gas, either by direct collisions (Davidson & McCray 1980;Brown et al 1991) or through photoionization by extreme ultraviolet and X-ray photons produced in shocks and subsequent collisional ionization and excitation by suprathermal electrons (Begelman et al 1980).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Collimated radiation in SS 433

Waisberg

Dexter

Olivier-Petrucci

et al. 2019

A&A

View full text Add to dashboard Cite

Context. The microquasar SS 433 is well known for its precessing, relativistic, and highly collimated baryonic jets, which manifest in its optical spectrum as pairs of hydrogen and helium emission lines moving with large Doppler shifts. Depending on their heating mechanism, the optical jet bullets may serve as a probe of the collimated radiation coming from the inner region close to the compact object, and which is not directly visible to observers on Earth. Aims. We aim to better understand the baryonic jet phenomenon in SS 433, in particular the properties of the optical bullets and their interaction with the ionizing collimated radiation. Methods. The optical interferometer VLTI/GRAVITY has allowed us to spatially resolve the optical jets in SS 433 for the first time. We present here the second such observation taken over three nights in July 2017. In addition, we used the X-shooter spectrograph at VLT to study the optical bullets in SS 433 in detail. Over the full wavelength range 0.3−2.5 μm, we identified up to twenty pairs of jet lines observed simultaneously, which we modeled with the spectral synthesis code Cloudy. Results. GRAVITY reveals elongated exponential-like radial spatial profiles for the optical jets on scales ≲1−10 mas, suggestive of a heating mechanism acting throughout a long portion of the jet and naturally explained by photoionization by the collimated radiation. We also spatially resolve the movement of the optical bullets for the first time, detecting more extended jet components corresponding to previous ejections. Cloudy photoionization models can explain the spatial intensity profiles measured with GRAVITY and the emission line ratios from X-shooter, and constrain the properties of the optical bullets and the ionizing radiation. We find that the latter must peak in the UV with an isotropic luminosity (as inferred by a face-on observer) ∼1041 erg s−1. Provided that the X-ray spectral energy distribution is sufficiently hard, the collimated X-ray luminosity could still be high enough so that the face-on observer would see SS 433 as ultraluminous X-ray source and it would still be compatible with the H/He/He+ ionization balance of the optical bullets. The kinetic power in the optical jets is constrained to 2−20 × 1038 erg s−1, and the extinction in the optical jets to AV = 6.7 ± 0.1. We suggest there may be substantial AV ≳ 1 and structured circumstellar extinction in SS 433, likely arising from dust formed in equatorial outflows.

show abstract

Section: Collimated Radiationsupporting

confidence: 90%

Section: Resultsmentioning

confidence: 82%

Section: Cloudy Models For Photoionized Optical Bulletsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Collimated radiation in SS 433

Waisberg

Dexter

Olivier-Petrucci

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…tempts to estimate them indirectly (e.g. Panferov & Fabrika 1993;Medvedev & Fabrika 2010). We assume that SS 433 'face-on' appearance is similar to ULXs (Fabrika et al 2015), i.e.…”

Section: Predicted Signalmentioning

confidence: 99%

Is SS 433 a misaligned ultraluminous X-ray source? Constraints from its reflected signal in the Galactic plane

Khabibullin¹,

Sazonov²

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We evaluate the emission that must arise due to reflection of the putative collimated X-ray radiation of SS 433 by atomic gas and molecular clouds in the Galactic plane and compare the predicted signal with existing RXTE and ASCA data for the region of interest. Assuming that the intrinsic X-ray spectrum of SS 433 is similar to that of ultraluminous X-ray sources (ULXs), we obtain an upper limit of ∼ 2 × 10 39 erg s −1 on its total (angular-integrated) luminosity in the 2-10 keV energy band, which is only weakly dependent on the half-opening angle, Θ r , of the emission cone. In contrast, the upper limit on the apparent luminosity of SS 433 (that would be perceived by an observer looking at its supercritical accretion disk face-on) decreases with increasing Θ r and is ∼ 3 × 10 40 erg s −1 for Θ r Θ p = 21 • , where Θ p is the precession angle of the baryonic jets (assuming that the emission cones precess in the same manner as the jets). This leaves open the possibility that SS 433 is a misaligned ULX. Further investigation of the reflection signal from the molecular clouds using higher angular resolution observations could improve these constraints with the potential to break the degeneracy between Θ r and the apparent luminosity.

show abstract

Investigating unusual Hα features towards the Scutum Supershell

Alsulami,

Einecke,

Rowell

et al. 2024

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

We investigate the unusual H $\alpha$ features found towards the Scutum Supershell via recent arc-minute and arc-second resolution imaging. These multi-degree features resemble a long central spine ending in a bow-shock morphology. We performed a multi–wavelength study in [S II] optical, radio continuum, infrared continuum, Hi, CO, X-ray, and gamma-ray emissions. Interestingly, we found the Galactic worm GW 16.9−3.8 Hi feature appears within the Scutum Supershell, and likely influences the spine morphology. Furthermore, the rightmost edge of the bow-shock H $\alpha$ emission overlaps with [S II] line emission, 4.85 GHz radio, and both 60 and 100 $\mu$ m infrared continuum emissions, suggesting some potential for excitation by shock heating. We estimated the photo-ionisation from O-type and B-type stars in the region (including those from the OB associations Ser OB1B, Ser OB2, and Sct OB3) and found that this mechanism could supply the excitation to account for the observed H $\alpha$ luminosity of the spine and bow-shock of $\sim$ 1–2 $\times 10^{36}\,\mathrm{erg\,s}^{-1}$ (d/2.5 kpc) $^2$ . Recent MHD simulations by Drozdov et al. (2022) demonstrate the potential for supernova events to drive outflow and bow-shock types of features of the same energetic nature and physical scale as the H $\alpha$ emission we observe here. While this clearly requires many supernova events over time, we speculate that one contributing event could have come from the presumably energetic supernova (hypernova) birth of the magnetar tentatively identified in the X-ray binary LS 5039.

show abstract

Analysis of Balmer Lines Intensities and Radiation Non-Isotropy of SS 433 Jets

Cited by 9 publications

References 6 publications

Collimated radiation in SS 433

Collimated radiation in SS 433

Is SS 433 a misaligned ultraluminous X-ray source? Constraints from its reflected signal in the Galactic plane

Investigating unusual Hα features towards the Scutum Supershell

Contact Info

Product

Resources

About